Evolution of the Radio-X-Ray Coupling Throughout an Entire Outburst of Aquila X-1

Miller-Jones, J. C. A.; Sivakoff, G. R.; Altamirano, D.; Tudose, V.; Migliari, S.; Dhawan, V.; Fender, R. P.; Garrett, M. A.; Heinz, Sebastian; Körding, Elmar; Krimm, H. A.; Linares, M.; Maitra, D.; Markoff, Sera; Paragi, Z.; Remillard, Ronald A.; Rupen, M. P.; Rushton, A.; Russell, D. M.; Sarazin, Craig L.; Spencer, R. E.

doi:10.1088/2041-8205/716/2/l109

Cited by 80 publications

(99 citation statements)

References 36 publications

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“…The association of compact radio jets and X-ray hard tails with a specific region of the source in the hardnessintensity diagram is well documented (Fender et al 2004;Migliari & Fender 2006;Migliari et al 2007;Fender et al 2009;Miller-Jones et al 2010). Both the radio emission and the strength of the hard tail become weaker at higher accretion rates.…”

Section: Introductionmentioning

confidence: 90%

The photon-index–time-lag correlation in black hole X-ray binaries

Reig

Kylafis

Papadakis

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We have performed a timing and spectral analysis of a set of black-hole binaries to study the correlation between the photon index and the time lag of the hard photons with respect to the soft ones. We provide further evidence that the timing and spectral properties in black-hole X-ray binaries are coupled. In particular, we find that the average time lag increases as the X-ray emission becomes softer. Although a correlation between the hardness of the X-ray spectrum and the time (or phase) lag has been reported in the past for a handful of systems, our study confirms that this correlated behaviour is a global property of black-hole X-ray binaries. We also demonstrate that the photon-index -time-lag correlation can be explained as a result of inverse Comptonization in a jet.

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Section: Introductionmentioning

confidence: 90%

The photon-index–time-lag correlation in black hole X-ray binaries

Reig

Kylafis

Papadakis

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…This flow is then dominated by advection in which a significant fraction of the energy is advected and not 3 The radio-vs.-X-ray luminosity diagram is constructed using data for GX 339-4 from Corbel et al (2003) and a distance of 8 kpc, for H 1743-322 from Table 1 of Coriat et al (2011) and distance of 8 kpc, and for V404 Cyg from Corbel et al (2008) and a distance 2.39 kpc. For the atoll NS binary Aql X-1, we use data from Miller-Jones et al (2010) and distance 5 kpc, and for 4U 1728-34 we use data from Migliari & Fender (2006) and distance 4.6 kpc.…”

Section: An Lmxb Powering a Jet?mentioning

confidence: 99%

X-ray follow-ups of XSS J12270-4859: a low-mass X-ray binary with gamma-rayFermi-LAT association

Martino

Belloni

Falanga

et al. 2013

A&A

124

137

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Context. XSS J1227.0-4859 is a peculiar, hard X-ray source recently positionally associated to the Fermi-LAT source 1FGL J1227.9-4852/2FGL J1227.7-4853. Multi-wavelength observations have added information on this source, indicating a low-luminosity lowmass X-ray binary (LMXB), but its nature is still unclear. Aims. To progress in our understanding, we present new X-ray data from a monitoring campaign performed in 2011 with the XMM-Newton, RXTE, and Swift satellites and combine them with new gamma-ray data from the Fermi and AGILE satellites. We complement the study with simultaneous near-UV photometry from XMM-Newton and with previous UV/optical and near-IR data. Methods. We analysed the temporal characteristics in the X-rays, near-UV, and gamma rays and studied the broad-band spectral energy distribution from radio to gamma rays. Results. The X-ray history of XSS J1227 over 7 yr shows a persistent and rather stable low-luminosity (6 × 10 33 d 2 1 kpc erg s −1 ) source, with flares and dips being peculiar and permanent characteristics. The associated Fermi-LAT source 2FGL J1227.7-4853 is also stable over an overlapping period of 4.7 yr. Searches for X-ray fast pulsations down to msec give upper limits to pulse fractional amplitudes of 15 − 25% that do not rule out a fast spinning pulsar. The combined UV/optical/near-IR spectrum reveals a hot component at ∼13 kK and a cool one at ∼4.6 kK. The latter would suggest a late-type K2−K5 companion star, a distance range of 1.4−3.6 kpc, and an orbital period of 7-9 h. A near-UV variability ( 6 h) also suggests a longer orbital period than previously estimated. Conclusions. The analysis shows that the X-ray and UV/optical/near-IR emissions are more compatible with an accretion-powered compact object than with a rotational powered pulsar. The X-ray to UV bolometric luminosity ratio could be consistent with a binary hosting a neutron star, but the uncertainties in the radio data may also allow an LMXB black hole with a compact jet. In this case, it would be the first associated with a high-energy gamma-ray source.

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“…To locate H 1743−322 with regards to the universal radio/X-ray correlation of black holes and neutron stars X-ray binaries, we also plot on Fig. 1 the data from the black holes GX 339-4 (Corbel et al, in prep), V404 Cyg (Gallo et al 2003;Corbel et al 2008), Swift J1753.5-0127 (Soleri et al 2010) and GRO J1655-40 and from the neutron stars Aql X-1 (Tudose et al 2009;Miller-Jones et al 2010) and 4U 1728-34 (Migliari & Fender 2006). Fig.…”

Section: Introductionmentioning

confidence: 99%

Accretion-outflow connection in the outliers of the “universal” radio/X-ray correlation

et al. 2010

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Abstract. In recent years, numerous efforts have been devoted to unravel the connection between accretion flow and jets in accreting compact objects. Here we report new constraints on these issues, through the long term study of the radio and X-ray behaviour of the black hole candidate H 1743−322. This source is known to be one of the "outliers" of the universal radio/X-ray correlation, i.e. a group of stellar mass accreting black holes displaying fainter radio emission for a given X-ray luminosity, than expected from the correlation. In this work we find, at high X-ray luminosity in the hard state, a tight radio/X-ray correlation with an unusual steep slope of b = 1.38 ± 0.03. This correlation then breaks below ∼ 5 × 10 −3 L E dd (M/10M ) −1 in X-rays and becomes shallower. When compared with radio/X-ray data from other black hole X-ray binaries, we see that the deviant points of H 1743−322 join the universal correlation and seem to follow it at low luminosity. Based on these results, we investigate several hypotheses that could explain both the b ∼ 1.4 slope and the transition toward the universal correlation.

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Evolution of the Radio-X-Ray Coupling Throughout an Entire Outburst of Aquila X-1

Cited by 80 publications

References 36 publications

The photon-index–time-lag correlation in black hole X-ray binaries

The photon-index–time-lag correlation in black hole X-ray binaries

X-ray follow-ups of XSS J12270-4859: a low-mass X-ray binary with gamma-rayFermi-LAT association

Accretion-outflow connection in the outliers of the “universal” radio/X-ray correlation

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